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Central Stars of Planetary Nebulae in Galactic Open Clusters: Providing additional data for the White Dwarf Initial-to-Final-Mass Relation

Published online by Cambridge University Press:  30 December 2019

Vasiliki Fragkou ,
Quentin A. Parker ,
Albert Zijlstra ,
Richard Shaw  and
Foteini Lykou
Vasiliki Fragkou
Affiliation:
The University of Hong Kong, Department of Physics, Hong Kong SAR, China emails: [email protected], [email protected], [email protected]
Quentin A. Parker
Affiliation:
The University of Hong Kong, Department of Physics, Hong Kong SAR, China emails: [email protected], [email protected], [email protected]
Albert Zijlstra
Affiliation:
The University of Manchester, Manchester, UK email: [email protected]
Richard Shaw
Affiliation:
Space Telescope Science Institute, Maryland, USA email: [email protected]
Foteini Lykou
Affiliation:
The University of Hong Kong, Department of Physics, Hong Kong SAR, China emails: [email protected], [email protected], [email protected]
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Abstract

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Accurate (< 10%) distances of Galactic star clusters allow a precise estimation of the physical parameters of any physically associated Planetary Nebula (PN) and also that of its central star (CSPN) and its progenitor. The progenitor’s mass can be related to the PN’s chemical characteristics and, furthermore, provides additional data for the widely used white dwarf (WD) initial-to-final mass relation (IFMR) that is crucial for tracing the development of both carbon and nitrogen in entire galaxies. To date, there is only one PN (PHR1315- 6555) confirmed to be physically associated with a Galactic open cluster (ESO 96 -SC04) that has a turn-off mass ∼2Mʘ. Our deep HST photometry was used for the search of the CSPN of this currently unique PN. In this work, we present our results.

Keywords

Planetary NebulaeOpen Clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 400 - 401
Copyright
© International Astronomical Union 2019 

References

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